English (United Kingdom)

https://curated-unify.zendy.io/wp-json/zendy-region/v1/featured_content/oa?rat=en

https://curated-unify.zendy.io/wp-json/zendy-region/v1/highlighted_journal/

Global: Zendy Plus annual

Presents the access of premium content as premium feature

Premium Content

Presents the keyphrase highlighting as premium feature

Keyphrase Highlighting

Presents the summarisation as premium feature

Summarisation

Insights

Presents the pdf analysis as premium feature

PDF Analysis

Presents the zaia usage as premium feature

ZAIA

Global: Zendy Tools annual

Global: Zendy Free Plan

Global: Zendy Tools monthly

Global: Zendy Plus monthly

Most planetary systems -- including our own -- are born within stellarclusters, where interactions with neighboring stars can help shape the systemarchitecture. This paper develops an orbit-averaged formalism to characterizethe cluster's mean-field effects as well as the physics of long-period stellarencounters. Our secular approach allows for an analytic description of thedynamical consequences of the cluster environment on its constituent planetarysystems. We analyze special cases of the resulting Hamiltonian, correspondingto eccentricity evolution driven by planar encounters, as well as hyperbolicperturbations upon dissipative disks. We subsequently apply our results to theearly evolution of our solar system, where the cluster's collective potentialperturbs the solar system's plane, and stellar encounters act to increase thevelocity dispersion of the Kuiper belt. Our results are two-fold: first, wefind that cluster effects can alter the mean plane of the solar system by$\lesssim1\deg$, and are thus insufficient to explain the $\psi\approx6\deg$obliquity of the sun. Second, we delineate the extent to which stellar flybysexcite the orbital dispersion of the cold classical Kuiper belt, and show thatwhile stellar flybys may grow the cold belt's inclination by the observedamount, the resulting distribution is incompatible with the data.Correspondingly, our calculations place an upper limit on the product of thestellar number density and residence time of the sun in its birth cluster,$\eta\,\tau\lesssim2\times10^4\,$Myr/pc$^3$.

Dynamics of Planetary Systems Within Star Clusters: Aspects of the Solar System's Early Evolution